GRB 140102A
GCN Circular 15877
Subject
GRB 140102A: TAOS early optical afterglow detection
Date
2014-02-23T01:09:24Z (12 years ago)
From
Ying-Tung Chen at ASIAA/TAOS <ytchen@asiaa.sinica.edu.tw>
Y. T. Chen, S. K. King, C. Y. Wen, K. Y. Huang, S. Y. Wang, M. Lehner and
TAOS team
We observed the field of the Swift GRB 140102A (Hagen et al., GCN 15653)
with TAOS 0.5-m telescope of Lulin observatory (Taiwan) starting on Jan., 2
(UT) 21:19:49, i.e., 2.2 minutes after the trigger.
We detected the fading optical afterglow at the time between few early
optical afterglow observations (Xu et al., GCN 15655; Guziy et al., GCN
15685; Yoshii et al. GCN 15778). The details of the photometry were listed
below.
DATE_T_START T0+ T_EXP MAG
(UT) sec sec R
2014-01-02 21:19:49 132 49 15.3+/-0.11
2014-01-02 21:20:38 181 49 15.7+/-0.15
2014-01-02 21:21:27 230 49 16.1+/-0.26
2014-01-02 21:22:16 279 49 (Upper Limit = 16.2)
The R-band magnitude of nearby USNOB1 stars have been used for calibration.
We note that a special filter (5000-7200 A) was used in TAOS telescopes.
GCN Circular 15778
Subject
GRB 140102A: MITSuME Akeno Optical observation
Date
2014-01-30T14:06:05Z (12 years ago)
From
Taketoshi Yoshii at Tokyo Tech <yoshii.t.ac@m.titech.ac.jp>
T. Yoshii, Y. Saito, S. Kurita, Y. Tachibana, K. Ito, R. Usui, T.Tanigawa, Y. Yano,Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 140102A (L. M. Z. Hagen et al., GCN Circular #15653) with the
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.
The observation started on 2014-01-02 21:18:44 UT ( 67sec after the burst).
We detected the previously reported optical afterglow of GRB140102A (D. Xu et al., GCN Circular #15655) in the Ic band.
The measured magnitudes were listed below.
T0+ MID-UT T-EXP mag
----------------------------------------------------
67[sec] 21:18:59 30[sec] Rc = 14.36 $B!^(B 0.4 Ic = 13.01+/-0.17
----------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]
We used GSC2.3 catalog for flux calibration.
GCN Circular 15730
Subject
GRB 140102A: AAO optical upper limits
Date
2014-01-14T14:33:36Z (12 years ago)
From
Alina Volnova at SAI MSU <alinusss@gmail.com>
GRB 140102A: AAO optical upper limits
A. Volnova (IKI), R. Inasaridze (AAO), G. Inasaridze (AAO), V.
Zhuzhunadze (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 140102A (Hagen et al., GCN 15653) with
AS-32 (0.7m) telescope of Abastumani Observatory on Jan. 5 and 6. We
obtained several unfiltered images of 120 s exposure during each
observational set. On stacked images in the enhanced XRT circle (Goad
et al., GCN 15657) we do not detect the optical afterglow.
The details of the photometry are the following:
Date T_start t-t0, exp., Uplim
(UT) mid, d s 3 sigma
2014-01-05 00:48:24 2.13972 38x120 22.5
2014-01-06 01:04:20 3.18687 32x120 22.3
The photometry is based on the SDSS reference stars from Xu (GCN 15655)
using gri -> R transformations by Lupton 2005:
N SDSS_id R(Lupton)
1 J140740.98+011949.8 17.59
2 J140742.47+012010.4 17.51
GCN Circular 15690
Subject
GRB 140102A: Swift/UVOT Detection
Date
2014-01-06T03:33:36Z (12 years ago)
From
Mike Siegel at PSU/Swift MOC <siegel@swift.psu.edu>
L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 140102A 65 s
after the BAT trigger (Hagen et al., GCN Circ. 15653). We detect a fading
source consistent with the XRT position (Goad et al. GCN Circ. 15657) that
is detected in all but the bluest UVOT filters.
The preliminary UVOT position is:
RA (J2000) = 14:07:40.65 = 211.91939 (deg.)
Dec (J2000) = +01:19:59.8 = 1.33329 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).
Preliminary detections and 3-sigma upper limits using the UVOT photometric
system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white (fc) 65 215 147 16.07 +/- 0.03
white 557 2215 322 18.38 +/- 0.05
white 6222 7858 393 20.08 +/- 0.21
v 607 2265 194 18.21 +/- 0.23
b 533 2191 175 18.50 +/- 0.15
u (fc) 278 527 245 16.90 +/- 0.05
u 681 2166 155 17.97 +/- 0.14
w1 657 2142 175 19.10 +/- 0.33
m2 631 2117 175 >19.34
w2 6428 8034 364 >19.96
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 15689
Subject
LOAO R-band Observation of GRB 140102A
Date
2014-01-06T02:52:23Z (12 years ago)
From
Changsu Choi at Seoul Nat U <changsu@astro.snu.ac.kr>
Changsu Choi, Myungshin Im (CEOU/SNU), Hyun-Il Sung (KASI), and Yuji Urata
(NCU), on behalf of EAFON
We observed the field of GRB 140102A (Hagen et al., GCN 15653) in R-band
using the 1-m telescope at Mt. Lemmon Optical Observatory (LOAO) in Arizona,
US
The observation started at 2014-01-03 13:01:40 UT, or about 15.34 hours
after the BAT alert.
We marginally identify the afterglow in a stacked image with a total
exposure time of ~ 45min. The approximate magnitude of the object is R(Vega)
= 21.5 +- 0.3 mag, calibrated against R1-mag of USNO-B1 stars in the
vicinity.
We thank the LOAO operator, Jae-Hyuk Yoon for performing the observation.
GCN Circular 15685
Subject
GRB 140102A: BOOTES-4 early optical observations
Date
2014-01-05T15:29:18Z (12 years ago)
Edited On
2024-11-18T10:05:03Z (a year ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
S. Guziy (Nikolaev Univ. Obs., Ukraine), J. Gorosabel (UPV/EHU-IAA/CSIC,
Spain), A. J. Castro-Tirado, R. Cunniffe, M. Jelínek, S. Jeong, O.
Lara-Gil, R. Sánchez-Ramírez, J. C. Tello (IAA-CSIC Granada, Spain), P.
Kubánek FZU-CAS, Czech Rep.), S. B. Pandey (ARIES, India), Y. Fan, X.
Zhao, J. Bai, Ch. Wang, Y. Xin (Yunnan National Astronomical Observatory,
China) and Ch. Cui (Beijing National Astronomical Observatory, China), on
behalf of a larger collaboration, report:
"Following the detection of GRB 140102A by Swift (Hagen et al., GCNC
15653) and Fermi (Sonbas et al. GCNC 15659), the robotic 0.6m MET
telescope at the BOOTES-4 station, in Lijiang Astronomical Observatory
(China) responded to the event with the first images being obtained 30s
post-burst. At the position of the optical afterglow detected by
Swift/UVOT we detect a source
rapidly decaying in brightness, with R = 14.0 about 70s after the burst
trigger time. Detailed analysis of the whole BOOTES-4 dataset is ongoing."
[GCN OPS NOTE(07jan14): Per author's request, the "130102A" in the first line
was corrected to "140102A".]
GCN Circular 15677
Subject
GRB 140102A, Optical Observations
Date
2014-01-04T12:02:35Z (12 years ago)
From
Shashi Bhushan Pandey at ROTSE <shaship@umich.edu>
S.B. Pandey, Brajesh Kumar and Parveen Kumar (ARIES Nainital India, on
behalf of larger Indian GRB collaboration)
We observed GRB 140102A (Swift trigger 582760, Hagen et al. 2014,
GCNC 15653) field with the 1.3m telescope at ARIES, Nainital starting
~ 1.5 hours after the burst. Several frames in V,R_c and I_c pass-bands
were obtained in clear sky conditions.
The candidate optical afterglow (Hagen et al. 2014, GCNC 15653; Xu et al.
2014, GCNC 15655) was clearly seen in our frames. The
photometry of the first R_c frame yields afterglow brightness to be ~ 19
mag.
The nearby USNO stars have been used for calibrate.
This massage may be cited.
GCN Circular 15674
Subject
GRB 140102A: P60 observations
Date
2014-01-03T21:35:47Z (12 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:
We imaged the location of Swift GRB 140102A (Hagen et al., GCN 15653),
also detected by the Fermi/LAT (Sonbas et al., GCN 15659) with the
Palomar 60-inch (P60) robotic telescope on UT 2014-01-03 between 12:01
and 12:45 UT, in the g, r, i, and z filters.
The afterglow is marginally detected in individual exposures, and
clearly detected after stacking all of the observations in each filter.
Photometry of the stacks relative to SDSS stars in the field gives
magnitudes (at a common midpoint of approximately 12:23 UT, t=0.63 days
after the trigger) of:
g = 22.08 +/- 0.10
r = 21.59 +/- 0.09
i = 21.37 +/- 0.10
[GCN OPS NOTE(07jan14): Changed the "130102A" in the first line
to "140102A".]
GCN Circular 15669
Subject
GRB 140102A: Fermi/GBM Observation
Date
2014-01-03T16:46:14Z (12 years ago)
From
Binbin Zhang at UAH <binbin.zhang@uah.edu>
Bin-Bin Zhang and Narayana Bhat (UAH/CSPAR) report on behalf of the Fermi GBM Team:
"At 21:17:37.81 UT on January 02 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 140102A (trigger 410390260/
140102887). This GRB also triggered Swift (Hagen et al. GCN 15653) and
Konus-Wind (Golenetskii et al, GCN 15667) and was detected by Fermi/LAT
(Sonbas et al. GCN 15659) and in several ground follow-up observations
(Xu et al GCN 15655; Gorosabel et al, GCN 15658; Kimura et al, GCN 15663
and Tanga et al, 15665). The GBM on-ground calculated location is consistent
with the Swift/XRT position and those obtained with follow-up observations.
The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location. The
initial angle from the LAT boresight was 47 deg from the Fermi/GBM
position.
The GBM light curve consists of two major bright overlapping peaks. The
duration (T90) of the burst was about 3.6 s (50-300 keV). The time-averaged
spectrum from T0+0.4 s to T0+4 s is best fit with a Band function with
Epeak = 186 +/- 5 keV, alpha = -0.71 +/- 0.02 and beta = -2.49 +/- 0.07.
The event fluence (10-1000 keV) in this time interval is
(1.78 +/- 0.03)E-05 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+1.98 s in the 10-1000 keV band is 49.7 +/- 0.5 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 15667
Subject
Konus-Wind observation of GRB 140102A
Date
2014-01-03T15:53:48Z (12 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long-duration GRB 140102A
(Swift-BAT trigger 582760: Hagen et al., GCN 15653, Barthelmy et al., GCN 15662;
Fermi LAT detection: Sonbas et al., GCN 15659;
MAXI/GCS detection: Kimura at al., GCN 15663)
triggered Konus-Wind at T0=76656.245 s UT (21:17:36.245).
The burst light curve shows a multi-peaked structure from ~T0-0.5 s to ~T0+4 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140102_T76656/
As observed by Konus-Wind, the burst
had a fluence of (2.0 � 0.2)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.192 s,
of (1.3 � 0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum (measured from T0 to T0+10.496 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.05 � 0.14,
the high energy photon index beta = -2.68 � 0.30,
the peak energy Ep = 185 � 19 keV,
chi2 = 120/97 dof.
The spectrum near the maximum count rate
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.75 � 0.27,
the high energy photon index beta = -3.05 � 0.73,
the peak energy Ep = 200 � 31 keV,
chi2 = 85.8/69 dof.
All the quoted values are preliminary.
GCN Circular 15665
Subject
GRB 140102A: GROND observations
Date
2014-01-03T15:03:39Z (12 years ago)
From
Sylvio Klose at TLS Tautenburg <klose@tls-tautenburg.de>
M. Tanga (MPE Garching), S. Klose (TLS Tautenburg), and J. Greiner (MPE
Garching) report on behalf of the GROND team:
We observed the field of GRB 140102A (Hagen et al., GCN 15653)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile).
Observations started at 07:51 UT on Jan 03, about 10.5 hrs after the GRB
trigger. The afterglow discovered by Hagen et al. (see also Gorosabel et
al., GCN 15658; Xu et al., GCN 15655) is detected in all optical bands. At
a mean time of 08:19 UT, we measure the following preliminary AB
magnitudes:
g'= 21.6 +/- 0.1,
r'= 21.4 +/- 0.1,
i'= 20.9 +/- 0.1,
z'= 21.0 +/- 0.1,
J = 20.7 +/- 0.3,
H = 20.6 +/- 0.4,
K > 19.3,
calibrated against SDSS and 2MASS field stars.
After correcting for a Galactic reddening of E(B-V)=0.03 mag (Schlegel et
al. 1998), the spectral slope defined by g'r'z'JH is ~ 0.7, with no
evidence for host extinction.
The SED fit shows a slight excess in i'-band flux. It could be due to
emission line(s) from the underlying host, though we cannot say anything
about an underlying galaxy due to the bad image quality (FWHM ~ 2.5"). We
note, however, the presence of a galaxy just 4" East of the afterglow.
GCN Circular 15663
Subject
GRB 140102A: MAXI/GSC detection
Date
2014-01-03T14:11:53Z (12 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
M. Kimura (JAXA), T. Sakamoto (AGU), S. Nakahira (JAXA),
S. Ueno, H. Tomida, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, M. Serino, J. Sugimoto, T. Takagi,
A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, M. Sasaki, D. Uchida (Osaka U.),
H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.),
M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada, Y. Morooka (Miyazaki U.),
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:
The MAXI/GSC Nova alert system triggered a bright uncatalogued
X-ray transient source at 21:19:54 UT on 2014-01-02. Assuming that
the source flux was constant over the transit, we obtain the source position at
(R.A., Dec) = (211.813 deg, 1.477 deg) = (14 07 15, +01 28 37) (J2000)
with a statistical 90% C.L. elliptical error region in long and short radii of
0.46 deg and 0.35 deg respectively. The roll angle of long axis from the north
direction is 40.0 deg counterclockwise. There is an additional systematic
uncertainty of 0.1 deg (90% containment radius). This uncatalogued X-ray
source is temporary and positionally coincident with the Swift detected
GRB 140102A (Hagen et al. GCN #15653).
Using the data available from 21:16 to 21:23 UT, the MAXI/GSC spectrum
is created from T0(BAT)+58.2 sec to T0(BAT)+219.2 sec (T0(BAT) is the trigger
time of the Swift/BAT). An absorbed power-law model gives an acceptable
fit to the data. The best fit photon index is 2.7 (-0.8/+1.0). The unabsorbed
2-20 keV flux is 2.3 (-0.8/+0.9) x 10^-9 erg/cm2/s. All the quoted errors
are at the 90% confidence level.
There was no significant excess flux in the previous transit at
19:47 UT and in the next transit at 22:53 UT with an upper limit
of ~20 mCrab for each.
GCN Circular 15662
Subject
GRB 140102A, Swift-BAT refined analysis
Date
2014-01-03T14:07:40Z (12 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), L. M. Z. Hagen (PSU), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140102A (trigger #582760)
(Hagen, et al., GCN Circ. 15653). The BAT ground-calculated position is
RA, Dec = 211.915, 1.332 deg which is
RA(J2000) = 14h 07m 39.5s
Dec(J2000) = +01d 19' 54.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.
The mask-weighted light curve shows many overlapping peaks starting
at ~T-0.2 sec, peaking at ~T+0.7 sec and ending at ~T+5 sec with a long
tail emission out to T+200 sec. T90 (15-350 keV) is 65 +- 15 sec (estimated
error including systematics).
The time-averaged spectrum from T-0.15 to T+131.22 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.38 +- 0.04. The fluence in the 15-150 keV band is 7.7 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.97 sec in the 15-150 keV band
is 29.8 +- 0.6 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/582760/BA/
GCN Circular 15661
Subject
GRB 140102A: Swift-XRT refined Analysis
Date
2014-01-03T12:27:04Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U.
Leicester), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), P.
D'Avanzo (INAF-OAB) and L.M.Z. Hagen report on behalf of the Swift-XRT
team:
We have analysed 6.9 ks of XRT data for GRB 140102A (Hagen et al. GCN
Circ. 15653), from 47 s to 25.3 ks after the BAT trigger. The data
comprise 3.0 ks in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 15657).
The late-time light curve (from T0+5.4 ks) can be modelled with a
power-law decay with a decay index of alpha=1.72 (+0.16, -0.14).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+/-0.03). The
best-fitting absorption column is 1.31 (+/-0.09) x 10^21 cm^-2, in
excess of the Galactic value of 2.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.93 (+0.17, -0.16)
and a best-fitting absorption column of 9.0 (+4.1, -3.7) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.8 x 10^-11 (4.6 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 9.0 (+4.1, -3.7) x 10^20 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index: 1.93 (+0.17, -0.16)
If the light curve continues to decay with a power-law decay index of
1.72, the count rate at T+24 hours will be 6.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-13 (3.2 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00582760.
This circular is an official product of the Swift-XRT team.
GCN Circular 15659
Subject
GRB 140102A: Fermi-LAT detection of a burst
Date
2014-01-03T12:02:52Z (12 years ago)
From
Eda Sonbas at NASA/GSFC <edasonbas@gmail.com>
E. Sonbas (Adiyaman Univ.), G. Vianello (Stanford University) and F. Longo
(University and INFN, Trieste) report on behalf of the Fermi-LAT team:
The Fermi Large Area Telescope (LAT) detected emission from GRB 140102A,
also detected by Swift (Hagen et al., GCN 15653) and GBM (trigger
140102887) at 21:17:37.64 UT on January 02, 2014.
The GRB was detected at high enough peak flux in the GBM detectors to
trigger an autonomous repoint of the spacecraft. The source was 47 deg from
the LAT boresight at the time of the trigger, and then was kept close to
the boresight of the LAT up to 1200 seconds after the trigger. It entered
again the LAT field of view from T0+3400 to T0+7000 s.
Only the first couple of hundreds seconds of LAT data have been processed.
They show an excess temporally and spatially correlated with the emission
detected by Swift and by the GBM with very high significance. More than 20
photons above 100 MeV and more than 5 photons above 1 GeV are observed
within the first ~650 seconds. The highest energy photon is a 8 GeV event
which is observed 520 seconds after the GBM trigger.
The best LAT on-ground location is found to be RA, Dec 211.88, 1.36 (J2000)
with an error radius of 0.25 deg (90% containment, statistical error only),
which is 0.05 deg from the afterglow candidate detected and localized by
Swift/UVOT (GCN 15653).
The Fermi LAT point of contact for this burst is Eda Sonbas (
edasonbas@yahoo.com).
The Fermi LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an
international collaboration between NASA and DOE in the U.S. and many
scientific institutions across France, Italy, Japan and Sweden.
GCN Circular 15658
Subject
GRB 140102A: I-band observations from IAC80 and 1.23m CAHA telescopes
Date
2014-01-03T09:15:08Z (12 years ago)
From
Javier Gorosabel at IAA-CSIC <jgu@iaa.es>
J. Gorosabel (IAA/CSIC-UPV/EHU), V. Terron (IAA/CSIC), E. Gomez (IAC), J. Cepa (IAC), M. Fernandez (IAA/CSIC), report on behalf of a larger collaboration:
We observed the GRB140102A optical afterglow (Hagen et al., GCN 15653; Xu et al., GCN 15655) in the I-band using the 1.23m CAHA and IAC80 telescopes. The images were acquired on Jan 3.2569-3.2670 UT and Jan 3.2719-3.2942 UT, respectively. The afterglow is clearly detected with I~20.5 (vega), calibrated against the USNO B1.0 catalog.
GCN Circular 15657
Subject
GRB 140102A: Enhanced Swift-XRT position
Date
2014-01-03T03:46:44Z (12 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2356 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140102A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 211.91916, +1.33314 which is equivalent
to:
RA (J2000): 14h 07m 40.60s
Dec (J2000): +01d 19' 59.3"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 15655
Subject
GRB 140102A: Early optical observations from Nanshan
Date
2014-01-03T00:07:27Z (12 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), X. Zhang, C.-H. Bai, H.-B. Niu, A. Esamdin, L. Ma
(XAO) report:
We observed the field of GRB 140102A (Hagen et al., GCN 15653) using
the 1m telescope located on Mt. Nanshan, Xinjiang, China, equipped
with a 1.2x1.2 deg^2 CCD camera. Observations started at 21:27:51 UT
on 2014-01-02 (i.e., 614s after the BAT trigger). All frames are in R
filter.
We find a decaying afterglow at the UVOT position, beginning with
R~16.3 mag at a mean time of 674s post-burst. The afterglow is
decaying roughly as F(t) ~ t^-1 up to ~7000s post-burst, possibly with
fluctuations in between. Observations are ongoing.
Photometry is calibrated with nearby stars: SDSS J140740.98+011949.8
and SDSS J140742.47+012010.4.
GCN Circular 15653
Subject
GRB 140102A: Swift detection of a burst with optical counterpart
Date
2014-01-02T21:27:38Z (12 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
S. B. Cenko (GSFC), D. Grupe (PSU), S. T. Holland (STScI),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU), T. N. Ukwatta (MSU)
and B.-B. Zhang (UAH) report on behalf of the Swift Team:
At 21:17:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140102A (trigger=582760). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 211.902, +1.331 which is
RA(J2000) = 14h 07m 37s
Dec(J2000) = +01d 19' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a double-peaked
structure with a total duration of about 8 sec. The peak count rate
was ~55,000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 21:18:34.3 UT, 56.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 211.9190, 1.3333 which is equivalent to:
RA(J2000) = +14h 07m 40.56s
Dec(J2000) = +01d 19' 59.9"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 61 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 7.00e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 65 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 14:07:40.65 = 211.91936
DEC(J2000) = +01:19:59.7 = 1.33325
with a 90%-confidence error radius of about 0.74 arc sec. This position is 1.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.98 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03.
Burst Advocate for this burst is L. M. Z. Hagen (lea.zernow.hagen AT gmail.com).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)